Discussion on Coordinated Science Development Needed for HMI

C.4. SCIENCE TEAM - notes from HMI proposal “There are two key aspects to the selection of a science team. First is to assure that the capabilities are present to complete the development of the flight program. No less important is the need to assure that those with the knowledge and capability to complete the science investigation are committed to the program. The HMI Science Team includes the Co-Investigators and other named individuals referred to as Associated Investigators (AI). The Science Team as a whole is dedicated to ensuring that the best possible science investigation is accomplished within the SDO-HMI program. The HMI Science Team consists of leading experts in all of the science goals of the HMI investigation.

In Phase D a number of Co-Is will provide software for use in the level-1 through level-3 processing pipeline. This software will allow timely calibration of the data from the beginning of the flight phase and the production of higher level science data products required for later science analysis. These data products are those that require substantial volumes of data and processing that can not be expected to be available at Co-I and other science institutions. In the first two years of Phase-E (E-1) the Stanford, LMSAL, HAO, and international investigators will pursue their full science investigation as well as operations, data processing, calibration as appropriate.

The US Co-Is who provided code in Phase-D will participate in the calibration to ensure the proper functioning of the code and algorithms and will pursue a reduced science investigation - sufficient to verify that the algorithms developed yield the science insights intended. In the final years, Phase E-2, the Stanford and LMSAL investigators will continue their operations and processing roles but will pursue only similarly limited science investigations. The support for the full exploitation of the HMI science opportunities by US investigators during this phase must come from sources other than the primary HMI program. This plan is consistent with the requirements specified in the AO Section 1.6 paragraph 2. “

Table C.4.1 - Team Participation in Mission Phases D E-1 E-2 Stanford Full Ops, Data, Calib, Science Ops, Data, Some Science LMSAL Ops, Calib, Science Ops, Some Science MSSL Yes Science RAL HAO Line Sel. none Code Develop Calib, Science Other US Calib, Some Science Other Intl Table C.4.1 - Team Participation in Mission Phases

Note from Ken Schwer As mentioned at each of your Instruments SRRs and at the Mission SCR, we have additional Phase E funds for science analysis.  The original AO section 1.6 direction stated that ....Investigators should cost their Phase E efforts to provide for the entire analysis effort for their investigations during the first two years after launch.  Less funding will be provided for the selected investigations for subsequent years; in particular proposers should reduce their phase E budget by ~ 50% for the years three to six.  Additional science analyses using equivalent resources are expected to be completed in an LWS Guest Investigator program that will be advertised by NASA (TR&T or equiv.)…... The additional funding will be for on-orbit years 3-6 so that SDO Science analysis does not solely rely on the Guest Investigator program after year 2.  You will soon be directed by GSFC to include the additional cost/analyses in your B/C/D/E proposals.  Therefore, each Instrument team shall work with Tom Anderson & Barbara in order to identify which areas are appropriate for SDO $'s and which areas are better for proposing to TR&T $s.

Notes forwarded to the LWS-TR&T Definition Team as examples of SDO related investigations in need of coordinated TR&T support. “Important SDO research not specifically funded through the investigations. “There are irradiance models which need continuing development. The integration of the solar EUV irradiance and images with models such as the NRL EUV solar irradiance model is important research that will greatly benefit SDO science if some of this work can be done before SDO launches. This type research will directly benefit EVE and AIA measurements and could use existing TIMED SEE solar EUV irradiances and SOHO EIT images as a test-bed for SDO.

“Coronal field models - working towards a treatment like the SEC Arge model (daily update with solar wind predictions) More generally there needs to be continued work on full Sun to Magnetosphere modeling. At present the CISM project is working on a full model. The Berkeley and Michigan MURI projects are working on data analysis oriented models vs. the more physics-only CISM plans. So long as CISM and MURI projects are ongoing the modeling efforts can be coordinated in cooperation with those projects. Additionally there is a need for assimilation models to be developed. An example is that in progress now by Schrijver et al. as part of LWS TR&T work. These modeling efforts are necessary for SDO. They are presently ongoing and need continued TR&T support.

“Local-area helioseismology development “Local-area helioseismology development. Including all non-global methods. Background: In the development phases of SOHO/MDI and GONG a significant research effort was focused on developing inversion techniques with known properties. This was done by developing solar models, making test sets of frequencies from the run of sound speed in those models with various perturbations, then applying test inversion methods to examine their sensitivity to solar model parameters, to the perturbations, and their noise and error characteristics. When data became available the inversions could be done with a reasonable degree of confidence in the inferences about the solar interior. Local-area helioseismology needs a similar coordinated development including numerical simulations of convective flows, either generating or embedding wave fields in those flows, “observing” these wave fields at the “surface”, then applying the various analysis techniques to test their effectiveness and the soundness of inferences made with them.

“This and other studies will allow exploitation of the data anticipated from SDO. This is beyond the scope of HMI development. Efforts are needed to improve and inter-compare complementary imaging techniques, evaluate their random and systematic errors, increase their spatial and temporal resolution, extend them to greater depths, extend far-side imaging closer to the solar limb and explore its predictive power, establish a baseline of lower resolution sub-surface weather images & explore their predictive power, advance modeling and theory of large and small scale sub-surface dynamics. “Much of this work can be done by analysis of SOHO/MDI, GONG+, and Mt Wilson datasets. Progress is underway on these topics with support from LWS TR&T, SRT, SOHO-GI, and SOHO/MDI grants but without coordination or guarantee that the results will be available in time for SDO.

“Vector magnetograph measurements of highly potential (erupting) compact fields & integration into existing CME models. This is more generally the topics once considered for the HAO Solar Magnetic Initiative. How magnetic fields are formed, move through the atmosphere, etc. These topics span HMI and AIA and many other missions and projects. But in particular advance work needs to be done to accomplish the SDO goals that span instruments.”